Shape and position of Earth's bow shock near-lunar orbit based on ARTEMIS data  

作　　者：LIU Ji SHI QuanQi TIAN AnMin Lü JianYong WU Hao WANG Ming FU SuiYan YANG YuChen ZONG QiuGang ZHANG Jiang FENG YongYong PU ZuYin 

机构地区：[1]School of Space Science and Physics,Shandong University,Weihai 264209,China [2]State Key Laboratory of Space Weather,Chinese Academy of Sciences,Beijing 100190,China [3]Institute of Space Weather,Nanjing University of Information Science and Technology,Nanjing 210044,China [4]School of Earth and Space Sciences,Peking University,Beijing 100871,China

出　　处：《Science China Earth Sciences》2016年第8期1700-1706,共7页中国科学（地球科学英文版）

基　　金：supported by the National Natural Science Foundation of China(Grant Nos.41322031,41404131,41574157,41031065&41304129);the Specialized Research Fund for State Key Laboratories;the Shandong Natural Science Foundation(Grant Nos.2013BSE27132,BS2013HZ001)

摘　　要：Earth's bow shock is the result of interaction between the supersonic solar wind and Earth's magnetopause. However, data limitations mean the model of the shape and position of the bow shock are based largely on near-Earth satellite data. The model of the bow shock in the distant magnetotail and other factors that affect the bow shock, such as the interplanetary magnetic field(IMF) B_y, remain unclear. Here, based on the bow shock crossings of ARTEMIS from January 2011 to January 2015, new coefficients of the tail-flaring angle a of the Chao model(one of the most accurate models currently available) were obtained by fitting data from the middle-distance magnetotail(near-lunar orbit, geocentric distance -20R_E>X>-50R_E). In addition, the effects of the IMF B_y on the flaring angle a were analyzed. Our results showed that:(1) the new fitting coefficients of the Chao model in the middle-distance magnetotail are more consistent with the observed results;(2) the tail-flaring angle a of the bow shock increases as the absolute value of the IMF B_y increases. Moreover, positive IMF B_y has a greater effect than negative IMF B_y on flaring angle. These results provide a reference for bow shock modeling that includes the IMF B_y.Earth’s bow shock is the result of interaction between the supersonic solar wind and Earth’s magnetopause. However, data limitations mean the model of the shape and position of the bow shock are based largely on near-Earth satellite data. The model of the bow shock in the distant magnetotail and other factors that affect the bow shock, such as the interplanetary magnetic field（IMF） B_y, remain unclear. Here, based on the bow shock crossings of ARTEMIS from January 2011 to January 2015, new coefficients of the tail-flaring angle a of the Chao model（one of the most accurate models currently available） were obtained by fitting data from the middle-distance magnetotail（near-lunar orbit, geocentric distance -20R_E〉X〉-50R_E）. In addition, the effects of the IMF B_y on the flaring angle a were analyzed. Our results showed that：（1） the new fitting coefficients of the Chao model in the middle-distance magnetotail are more consistent with the observed results;（2） the tail-flaring angle a of the bow shock increases as the absolute value of the IMF B_y increases. Moreover, positive IMF B_y has a greater effect than negative IMF B_y on flaring angle. These results provide a reference for bow shock modeling that includes the IMF B_y.

关 键 词：Bow shock Interplanetary magnetic field(IMF) MAGNETOSPHERE Solar wind 

分 类 号：P353[天文地球—空间物理学]